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We estimated the coronal magnetic field strength ($B$) during the 23 July2016 coronal mass ejection (CME) event using i) the flux rope structure of theCME in the whitelight coronagraph images and ii) the band splitting in theassociated type {\sc II} burst. No models were assumed for the coronal electrondensity ($N(r)$) used in the estimation.The results obtained using the abovetwo independent methods correspond to different heliocentric distances ($r$) inthe range $\approx$\,2.5\,--\,4.5$\rm R_{\odot}$, but they show excellentconsistency and could be fitted with a single power-law distribution of thetype $B(r)=5.7r^{-2.6}$ \textrm{G}, which is applicable in the aforementioneddistance range. The power law index i.e. $-2.6$) is in good agreement with theresults obtained in previous studies by different methods.

Strength of the Solar Coronal Magnetic field - A Comparison of Independent Estimates Using Contemporaneous Radio and White-light Observations